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LH54-425
LH54-425 is a star system that was identified as a spectroscopic binary by astronomer Pablo G. Ostrov in 2002. It is located in the LH 54 OB association within the Large Magellanic Cloud〔 Both members are O-type stars and the pair is among the most massive known. They are emitting a stellar wind with a velocity of 2,800 km/s.〔 As the pair evolve, they may merge to form a single star with a mass 80 times that of the Sun. In time, they will explode as a core-collapse supernova.〔 ==References==
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